SIMBAD references

Using the phat-ELVIS suite of Milky Way-sized halo simulations, we show that subhalo orbital pericentres, r_peri, correlate with their dark matter halo structural properties. Specifically, at fixed maximum circular velocity, V_max, subhaloes with smaller r_peri are more concentrated (have smaller r_max values) and have lost more mass, with larger peak circular velocities, V_peak, prior to infall. These trends provide information that can tighten constraints on the inferred V_max and V_peak values for known Milky Way satellites. We illustrate this using published pericentre estimates enabled by Gaia for the nine classical Milky Way dwarf spheroidal satellites. The two densest dSph satellites (Draco and Ursa Minor) have relatively small pericentres, and this pushes their inferred r_max and V_max values lower than they would have been without pericentre information. For Draco, we infer V_ max_ = 23.5 ±3.3 km s^–1 (compared to 27.3 ±7.1 km s^–1 without pericentre information). Such a shift exacerbates the traditional Too Big to Fail problem. Draco's peak circular velocity range prior to infall narrows from V_peak = 21-51 km s^–1 without pericentre information to V_peak = 25-37 km s^–1 with the constraint. Over the full population of classical dwarf spheroidals, we find no correlation between V_peak and stellar mass today, indicative of a high level of stochasticity in galaxy formation at stellar masses below ∼10⁷ M_☉. As proper motion measurements for dwarf satellites become more precise, they should enable useful priors on the expected structure and evolution of their host dark matter subhaloes.